星系團的重子質量比之二維投影分佈圖

Abstract

我們提出了一個新方法來製造星系團的重子質量比之二維投影分佈圖。在這個研究裡我們直接使用了 AMiBA13 的 SZ 效應和哈伯天文望遠鏡的重力透鏡效應觀測結果以及以X光觀測的星系團溫度。另外我們比較了實際上觀測的結果與用理論模型估算結果之間的差異。此方法能夠讓我們直接看出星系團的重子質量比在圖上的分佈情況，並且從結果得知我們提出的新方法與實際觀測結果得到的影像品質有直接的關係，若能提高觀測的解析度與視野大小，或是排除觀測結果中的雜訊干擾及造成誤差的因素，此方法都將能呈現更詳細的結果。

We demonstrate a new method to produce the projected 2D baryonic-fraction maps of galaxy clusters. In this work, the projected 2D baryonic-fraction maps are obtained by processing the images from Sunyaev-Zel'dovich effect and the kappa maps from gravitational lensing directly. The data we use are from two sources: (1) Array for Microwave Background Anisotropy (AMiBA) Sunyaev-Zel'dovich effect observations and (2) results from gravitational lensing analysis in Canada France Hawaii Telescope (CFHT) data and Hubble Space Telescope (HST) data of the Cluster Lensing And Supernova survey with Hubble (CLASH) sample combined with X-ray temperature. For the purpose of facilitating comparison, we use numerical simulations to reconstruct the cold dark matter halo in the clusters with NFW model and the intracluster medium (ICM) with KS01 model.